Broad Energy-Band Ions in the Heliosphere and Their Coupling with Turbulence
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摘要: 围绕“日球层太阳风及其与侵入星际风的作用”这个主题，从目前认知、前沿问题、探测建议等3方面展开论述。日球层中的离子包括：原初太阳风离子、源于星际风的拾起离子、超热离子。其中拾起离子和超热离子有来自局地星际质侵入流的贡献。深空飞船探测到双模态遍布日球层：日球层内边界、太阳风、行星际湍动、超热离子能谱等都存在双模态特征。前沿问题有3个方面：①从未到达的领域，即黄道面里的日球层尾部以及高纬的外日球层；②曾经到达的领域，但是没有探测的物理量，例如外日球层中的拾起离子；③曾经到达并探测，但是形成机制不明，例如超热离子的幂律谱及其双模态。针对上述前沿问题，本文提出如下的建议：①设计不同的飞行路径，朝向不同的方位进行探测；②携带宽能段的离子谱仪器包涵盖原初太阳风等离子体、拾起离子和超热离子；③搭载高灵敏度磁强计测量外日球层的可压缩磁湍动。Abstract: This paper focuses on the theme of “solar wind in the heliosphere and its interaction with the invading interstellar wind”, and discusses it from three aspects: current cognition, frontier problems, and exploration suggestions. The ions in the heliosphere include primary solar wind ions, pick-up ions converted partially from interstellar wind, and super-thermal ions. Among them, pick-up ions and super-thermal ions have their contribution from the local interstellar medium flow. The deep-space spacecraft have detected the prevalence of two modes in the heliosphere: the inner boundary of the heliosphere, the solar wind, the interplanetary turbulence, and the energy spectrum of the super-thermal ions. There are three types of cutting-edge issues: ① the territory never reached, that is, the tail of the heliosphere in the ecliptic plane and the outer heliosphere at high latitudes; ② the territory that has been reached, but some key variables have not been detected, such as the picked-up ions in the outer heliosphere; ③ the territory and variables that have been reached and detected, but the formation mechanism is unknown, such as the power-law spectrum and dual-mode of the super-thermal ions. To address these problems, we put forward the following suggestions: ① to design different flight paths and detect in different directions; ② to carry ion spectra instruments with wide energy band, covering the primary solar wind plasma, the pick-up ions, and the super-thermal ions; ③ to carry high sensitivity magnetometer to measure the compressible magnetic turbulence in the outer heliosphere.
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Key words:
- outer heliosphere /
- interstellar wind /
- particle spectrum
Highlights● This paper points out that the broad energy-band ion spectrum and its coupling with the turbulence is one of the key windows to understand the interaction process between the heliosphere and the local interstellar medium. ● This work provides a brief review of the current cognition of the heliosphere, summarizes three related cutting-edge issues, and proposes the corresponding exploration suggestions for the future program. -
图 1 太阳系的时空坐标系
注：太阳系在时空坐标系下的三大重要科学命题：太阳系目前状态是什么（包括太阳风与星际介质相互作用到底如何）（淡红色云团及其中问号标记）、太阳系从哪儿来（太阳系的起源）（淡蓝色云团及其中问号标记）、太阳系将往何处去（太阳系的宿命）（淡绿色云团及其中问号标记）。
Fig. 1 The Solar system in the space-time coordinate system
图 2 5个维度的深空探测能力雷达图
Fig. 2 Five-dimensional deep space detection capability radar chart
图 4 “旅行者2号”飞船的日心距离、纬度随时间的变化
Fig. 4 The distance and latitude of the Voyager 2 spacecraft change over time
图 5 “旅行者1号”飞船上CRS载荷探测不同能档高能粒子的微分通量密度随飞行时间的变化
Fig. 5 The differential flux density of the CRS payload on the Voyager 1 spacecraft detects high-energy particles with different energy levels as a function of flight time
图 6 日球层太阳风及其湍动的双模态
Fig. 6 The dual mode of the heliospheric solar wind and its turbulence
图 7 宽能段离子的相空间密度谱在低速流和高速流中的差异
Fig. 7 The difference between the phase space density spectrum of the wide-energy band ion in the low-speed path and the high-speed flow
图 8 日球层可能的形状
Fig. 8 The shape of the heliosphere under different local interstellar medium assumptions
图 9 “新视野号”飞船上SWAP载荷测量到的离子计数率随单位电荷能量的变化剖面
Fig. 9 The change profile of ion count rate with unit charge energy measured by SWAP load on New Horizons spacecraft
图 10 “旅行者号”飞船在不同年份对超热离子和能量粒子（宇宙线）的测量能谱与三维可压缩湍动的模拟结果
Fig. 10 The measured energy spectra of the hot ions and energetic particles（cosmic rays）of the Voyager spacecraft in different years and three dimention simulation results of compressible turbulence
表 1 针对外日球层太阳风与侵入星际介质流的宽能段粒子测量的探测
Table 1 Detection suggestion table for the measurement of wide-energy particles in the outer heliosphere solar wind and intrusive interstellar medium flow
载荷 能量范围 探测对象 可选方案 太阳风法拉第杯 10 eV～12 keV 原初太阳风离子（H+，He++） 法拉第杯（FC） 太阳风静电分析仪 100 eV～20 keV 原初太阳风离子；部分星际风拾起离子
（H+，He+）静电分析仪（ESA） 拾起离子质谱仪 5 eV～80 keV 星际风拾起离子（H+，He+，N+，O+）；
部分超热离子静电分析仪（ESA）+飞行时间技术
（TOF）+ 固态半导体（SSD）超热离子谱仪 30 keV～5 MeV 湍动加速的超热离子 （双层）固态半导体SSD 
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